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Atomic transition probability measurements for 364 lines of Ti II in the UVthrough near IR are reported. Branching fractions from data recorded using aFourier transform spectrometer and a new echelle spectrometer are combined withpublished radiative lifetimes to determine these transition probabilities. Thenew results are in generally good agreement with previously reported FTSmeasurements. Use of the new echelle spectrometer, independent radiometriccalibration methods, and independent data analysis routines enables a reductionof systematic errors and overall improvement in transition probability accuracyover previous measurements. The new Ti II data are applied to high resolutionvisible and UV spectra of the Sun and metal-poor star HD 84937 to derive new,more accurate Ti abundances. Lines covering a range of wavelength andexcitation potential are used to search for non-LTE effects. The Ti abundancesderived using Ti II for these two stars match those derived using Ti I andsupport the relative Ti/Fe abundance ratio versus metallicity seen in previousstudies.

Improved Ti II log(gf) Values and Abundance Determinations in the Photospheres of the Metal-Poor Star HD 84937